All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F1.eps}} \end{figure}$ Figure 1: Raw and smoothed ¹⁰Be data. The lower curves (left axis) give the raw (thin curve) and the 1-2-1 filtered 8-year-averaged data from Antarctica (Bard et al. 1997). The upper curves (right axis) show the raw and the 11-year smoothed yearly data from Greenland (Beer et al. 1990).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{6cm}{\includegraphics{H4688F2.eps}} \end{figure}$ Figure 2: The differential response function of ¹⁰Be to the two main species of galactic cosmic rays, protons and $\alpha$ -particles, for different values of the heliospheric modulation strength, $\Phi$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{6cm}{\includegraphics{H4688F3.eps}} \end{figure}$ Figure 3: Local production rate of ¹⁰Be in the atmosphere as a function of the heliospheric modulation strength, $\Phi$ for different values of the local rigidity cutoff, $P_{\rm c}$ as denoted next to curves.
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In the text

$\begin{figure} \par\resizebox{6.5cm}{!}{\includegraphics{H4688F4.eps}} \end{figure}$ Figure 4: Scatter plot of 11-year averaged $\langle N^2 \rangle$ vs. $\langle N\rangle ^2$ based upon the yearly group sunspot numbers for 1700-2000. The regression line has a slope of $1.32\pm 0.01$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F5.eps}} \end{figure}$ Figure 5: 11-year averaged sunspot numbers for the last 400 years: group sunspot numbers (GSN), Wolf sunspot numbers (WSN), SN reconstructed from Greenland ¹⁰Be and SN reconstructed from 1-2-1 filtered Antarctic ¹⁰Be data. The shaded area roughly indicates the range of averaged SN for which the model is less reliable.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{5.2cm}{\includegraphics{H4688F6.eps}} \end{figure}$ Figure 6: Sunspot activity (11-year averaged) during the pre-instrumental era: earlier extrapolations by Schove (1955 - S55), Nagovitsyn (1997 - N97) and Rigozo et al. (2001 - R01), and our SN reconstructions from 1-2-1 filtered 8-year Antarctic (An) and from 11-year averaged Greenland (Gr) ¹⁰Be series. The shaded area indicates the range of averaged SN for which the applicability of the model is limited. Horizontal bars with arrows denote the known grand minima and maxima: Maunder minimum (Mm), Spörer minimum (Sm), Wolf minimum (Wm), Oort minimum (Om) and the Medieval maximum (MM). The shaded area roughly indicates the range of averaged SN for which the model is less reliable.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F7.eps}} \end{figure}$ Figure 7: Autocorrelation function of the measured SN (group, GSN, and Wolf, WSN) and the reconstructed (from Greenland and Antarctic ¹⁰Be data) sunspot series. Left panel: autocorrelation function for the period 1700-2000 (1700-1900 for the Antarctic series; 1700-1985 for the Greenland series). Right panel: autocorrelation function for the period after 850 for the Antarctic series and after 1424 for the Greenland series. Error bars represent the 95% confidence interval.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F8.eps}} \end{figure}$ Figure 8: FFT power spectra of the group sunspot number (GSN) series (1700-2000) as well as the sunspot number as reconstructed from the Antarctic (850-1900) and Greenland (1425-1980) ¹⁰Be series, from top to bottom respectively. Dotted lines indicate the corresponding 95% confidence intervals.
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In the text

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics{H4688F9.eps}} \end{figure}$ Figure 9: Variation of the parameters of the geomagnetic dipole during 850-2000 AD. Migration of the dipole axis (top panel, in geographical coordinates) and change of the virtual dipole moment M (lower panel).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F10.eps}} \end{figure}$ Figure 10: Global production rate of ¹⁰Be in the atmosphere as a function of the virtual geomagnetic dipole moment, M, for different values of the modulation strength, $\Phi$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F11.eps}} \end{figure}$ Figure 11: 11-year-averaged sunspot group sunspot number series (GSN) and the reconstructed SN for local and global ¹⁰Be deposition are represenetd by grey, solid, and dotted curves, respectively.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F1.eps}} \end{figure}$	Figure 1: Raw and smoothed ¹⁰Be data. The lower curves (left axis) give the raw (thin curve) and the 1-2-1 filtered 8-year-averaged data from Antarctica (Bard et al. 1997). The upper curves (right axis) show the raw and the 11-year smoothed yearly data from Greenland (Beer et al. 1990).
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{6cm}{\includegraphics{H4688F2.eps}} \end{figure}$	Figure 2: The differential response function of ¹⁰Be to the two main species of galactic cosmic rays, protons and $\alpha$ -particles, for different values of the heliospheric modulation strength, $\Phi$ .
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{6cm}{\includegraphics{H4688F3.eps}} \end{figure}$	Figure 3: Local production rate of ¹⁰Be in the atmosphere as a function of the heliospheric modulation strength, $\Phi$ for different values of the local rigidity cutoff, $P_{\rm c}$ as denoted next to curves.
Open with DEXTER

$\begin{figure} \par\resizebox{6.5cm}{!}{\includegraphics{H4688F4.eps}} \end{figure}$	Figure 4: Scatter plot of 11-year averaged $\langle N^2 \rangle$ vs. $\langle N\rangle ^2$ based upon the yearly group sunspot numbers for 1700-2000. The regression line has a slope of $1.32\pm 0.01$ .
Open with DEXTER

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F5.eps}} \end{figure}$	Figure 5: 11-year averaged sunspot numbers for the last 400 years: group sunspot numbers (GSN), Wolf sunspot numbers (WSN), SN reconstructed from Greenland ¹⁰Be and SN reconstructed from 1-2-1 filtered Antarctic ¹⁰Be data. The shaded area roughly indicates the range of averaged SN for which the model is less reliable.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F8.eps}} \end{figure}$	Figure 8: FFT power spectra of the group sunspot number (GSN) series (1700-2000) as well as the sunspot number as reconstructed from the Antarctic (850-1900) and Greenland (1425-1980) ¹⁰Be series, from top to bottom respectively. Dotted lines indicate the corresponding 95% confidence intervals.
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$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics{H4688F9.eps}} \end{figure}$	Figure 9: Variation of the parameters of the geomagnetic dipole during 850-2000 AD. Migration of the dipole axis (top panel, in geographical coordinates) and change of the virtual dipole moment M (lower panel).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F10.eps}} \end{figure}$	Figure 10: Global production rate of ¹⁰Be in the atmosphere as a function of the virtual geomagnetic dipole moment, M, for different values of the modulation strength, $\Phi$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{H4688F11.eps}} \end{figure}$	Figure 11: 11-year-averaged sunspot group sunspot number series (GSN) and the reconstructed SN for local and global ¹⁰Be deposition are represenetd by grey, solid, and dotted curves, respectively.
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